2012MNRAS.426.1291S

I measure the physical properties of 38 transiting extrasolar planetary systems, bringing the total number studied within the Homogeneous Studies project to 82. Transit light curves are modelled using the JKTEBOP code, with careful attention paid to limb darkening, orbital eccentricity and contaminating light. The physical properties of each system are obtained from the photometric parameters, published spectroscopic measurements and five sets of theoretical stellar model predictions. Statistical errors are assessed using Monte Carlo and residual permutation algorithms and propagated via a perturbation algorithm. Systematic errors are estimated from the interagreement between results calculated using five theoretical stellar models.

The headline result is a major upward revision of the radius of the planet in the OGLE-TR-56 system, from 1.23-1.38 to 1.734±0.051±0.029R_Jup (statistical and systematic errors, respectively). Its density is three times lower than previously thought. This change comes from the first complete analysis of published high-quality photometry. Significantly larger planetary radii are also found for Kepler-15, KOI-428, WASP-13, WASP-14 and WASP-21 compared to previous work.

I present the first results based on Kepler short-cadence data for Kepler-14, Kepler-15 and KOI-135. More extensive long-cadence data from the Kepler satellite are used to improve the measured properties of KOI-196, KOI-204, KOI-254, KOI-423 and KOI-428. The stellar component in the KOI-428 system is the largest known to host a transiting planet, at 2.48±0.17±0.20R_☉. Detailed analyses are given for HAT-P-3, HAT-P-6, HAT-P-9, HAT-P-14 and WASP-12, based on more extensive data sets than considered in previous studies.

Detailed analyses are also presented for the CoRoT systems 17, 18, 19, 20 and 23; Kepler-7, -12 and -17; KOI-254; OGLE-TR-111, -113, -132 and L9 and TrES-4.

I revisit the correlations between orbital period and surface gravity, and orbital period and mass of the transiting planets, finding both to be significant at the 4σ level. I conclude by discussing the opportunities for follow-up observations, the sky positions and the discovery rate of the known transiting planets.